BINARY STAR ORBITS. IV. ORBITS OF 18 SOUTHERN INTERFEROMETRIC PAIRS

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1 The Astronomical Journal, 140: , 2010 September C The American Astronomical Society. All rights reserved. Printed in the U.S.A. doi:1088/ /140/3/735 BIARY STAR ORBITS. IV. ORBITS OF 18 SOUTHR ITRFROMTRIC PAIRS Brian D. Mason 1,3, William I. Hartkopf 1,3, and Andrei Tokovinin 2 1 U.S. aval Observatory, 3450 Massachusetts Avenue, W, Washington, DC , USA; bdm@usno.navy.mil, wih@usno.navy.mil 2 Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile; atokovinin@ctio.noao.edu Received 2010 April 23; accepted 2010 June 25; published 2010 August 5 ABSTRACT First orbits are presented for 3 interferometric pairs and revised solutions for 15 others, based in part on first results from a recently initiated program of speckle interferometric observations of neglected southern binaries. ight of these systems contain additional components, with multiplicity ranging up to 6. Key words: binaries: close stars: individual (42 Cet, 36 Ser, β Sco, V505 Sgr, 74 Aqr) 1. ITRODUCTIO AD W MASURS While binary stars in the northern hemisphere have been observed for many years on a regular basis using various highresolution techniques (e.g., Horch et al. 2010; Balega et al. 2007; Docobo et al. 2008; Hartkopf & Mason 2009; McAlister et al. 1996; Prieur et al. 2009), their southern counterparts have received more limited attention. A recent program using a new speckle camera (Tokovinin et al. 2010, henceforth Paper I) has been undertaken to rectify this situation. Initial efforts have concentrated on observing pairs judged to require only a small amount of additional data in order to determine either first orbits or corrections to previously published elements seen to be in need of improvement. In this paper, we present the first sets of orbital elements to result from these data. In addition to the published measures from Paper I and earlier measures tabulated in the Washington Double Star (WDS; Mason et al. 2001) database, a significant number of measures for these pairs come from various previously unpublished sources. These included re-reductions or unpublished CHARA speckle interferometry data (see Hartkopf et al. 2000), unpublished USO speckle data (see Mason et al. 2009), and observations recently obtained with HRCam (as described in Paper I). These unpublished data are listed in Table 1. In this table, the first column gives the epoch-2000 coordinate, which is the primary identifier from the WDS. Columns 2 and 3 list the discoverer designation and an alternate designation, respectively. Column 4 lists the epoch of the observation expressed as a fractional Besselian year, and Columns 5 and 6 give the measured position angle (θ) and angular separation (ρ). ote that while equinox-200 coordinates are provided, position angles have not been corrected for precession and are thus based upon the equinox for the epoch of observation. Column 7 provides the characteristics of the filter used in the observation (central wavelength/fwhm, in nanometers) when known. The final column gives the aperture of the telescope in meters where the observation was obtained. This also uniquely defines the telescope: either the 4.2 m SOAR, the 4.0 m Blanco, the 3.8 m Mayall, or the 2.5 m Mt. Wilson Hooker telescope. Data obtained prior to 2001 were obtained with the CHARA speckle camera (Hartkopf et al. 2001), those after 2008 with HRCam (Paper I), and all other data with the USO speckle camera (Mason et al. 2009). 3 Visiting Astronomer, Kitt Peak ational Observatory and Cerro Tololo Inter-American Observatory. KPO and CTIO are operated by AURA, Inc. under contract to the ational Science Foundation. 2. W ORBITAL SOLUTIOS All orbits were either corrected or their first orbits attempted using the grid search routine described in Hartkopf et al. (1989); weights are applied based on the methods described by Hartkopf et al. (2001). lements for these systems are given in Table 2, where Columns 1 and 2 give the WDS and discoverer designations (followed by an alternate designation) and Columns 3 9 list the seven Campbell elements: P (period, in years), a (semimajor axis, in arcseconds), i (inclination, in degrees), Ω (longitude of node, equinox 200, in degrees), T 0 (epoch of periastron passage, in fractional Besselian year), e (eccentricity), and ω (longitude of periastron, in degrees). Formal errors are listed below each element. Columns 10 and 11 provide the orbit grade (see Hartkopf et al. 2001) and weighted rms residuals in θ and ρ for all measures used in the solution. Columns 12 and 13 give the reference for a previous orbit determination, if one exists, and weighted rms residuals in θ and ρ for that solution. Columns 11 and 13 are included in part to allow a more objective numerical comparison of the new and old solutions, in addition to the visual comparison provided by the figures. A quick inspection of Table 2 will reveal that half of these new pairs were first resolved by W. S. Finsen with his eyepiece interferometer. While these lower accuracy data are of less value in refining orbits, many of these pairs would not have been observed in the first place were it not for the monumental observing effort made by this great South African visual interferometrist. Figures 1 4 illustrate the new orbital solutions plotted together with all published data in the WDS database as well as the unpublished data in Table 1. In each of these figures, micrometric observations are indicated by plus signs, modern interferometric measures by filled circles, and older eyepiece interferometry measures by open circles; Hipparcos measures are indicated by the letter H. O C lines connect each measure to its predicted position along the new orbit (shown as a thick solid line). Dashed O C lines indicate measures given zero weight in the final solution. A dot-dashed line indicates the line of nodes, and a curved arrow in the lower right corner of each figure indicates the direction of orbital motion. Finally, the previous published orbit (when one exists) is shown as a dashed ellipse. The source of that orbit is listed in the 12th column of Table 2. Table 3 gives ephemerides for each new orbit over the years 2010 through 2015 in annual increments. Columns 1 and 2 are the same identifiers as in the previous table, while Columns 735

2 Report Documentation Page Form Approved OMB o Public reporting burden for the collection of information is estimated to average 1 hour per response, including the time for reviewing instructions, searching existing data sources, gathering and maintaining the data needed, and completing and reviewing the collection of information. Send comments regarding this burden estimate or any other aspect of this collection of information, including suggestions for reducing this burden, to Washington Headquarters Services, Directorate for Information Operations and Reports, 1215 Jefferson Davis Highway, Suite 1204, Arlington VA Respondents should be aware that notwithstanding any other provision of law, no person shall be subject to a penalty for failing to comply with a collection of information if it does not display a currently valid OMB control number. 1. RPORT DAT SP RPORT TYP 3. DATS COVRD to TITL AD SUBTITL Binary Star Orbits. IV. Orbits of 18 Southern Interferometric Paris 5a. COTRACT UMBR 5b. GRAT UMBR 5c. PROGRAM LMT UMBR 6. AUTHOR(S) 5d. PROJCT UMBR 5e. TASK UMBR 5f. WORK UIT UMBR 7. PRFORMIG ORGAIZATIO AM(S) AD ADDRSS(S) U.S. aval Observatory,3450 Massachusetts Avenue, W,Washington,DC, PRFORMIG ORGAIZATIO RPORT UMBR 9. SPOSORIG/MOITORIG AGCY AM(S) AD ADDRSS(S) 10. SPOSOR/MOITOR S ACROYM(S) 12. DISTRIBUTIO/AVAILABILITY STATMT Approved for public release; distribution unlimited 13. SUPPLMTARY OTS 11. SPOSOR/MOITOR S RPORT UMBR(S) 14. ABSTRACT First orbits are presented for 3 interferometric pairs and revised solutions for 15 others, based in part on first results from a recently initiated program of speckle interferometric observations of neglected southern binaries. ight of these systems contain additional components, with multiplicity ranging up to SUBJCT TRMS 16. SCURITY CLASSIFICATIO OF: 17. LIMITATIO OF ABSTRACT a. RPORT unclassified b. ABSTRACT unclassified c. THIS PAG unclassified Same as Report (SAR) 18. UMBR OF PAGS 9 19a. AM OF RSPOSIBL PRSO Standard Form 298 (Rev. 8-98) Prescribed by ASI Std Z39-18

3 736 MASO, HARTKOPF, & TOKOVII Vol. 140 Table 1 ew Speckle Interferometric Measures WDS or Discoverer Other Date θ ρ λ/δλ Tel α,δ (2000) Designation Designation (BY) ( ) ( ) (nm) (m) FI 337 BC 42 Cet / / FI 309 HD / CHR Ser / / / / / FI 336 HD / / / / HDS 3053 HD / / FI Psc / 4.2 (3+4), (5+6),...,and (13+14) give predicted values of θ and ρ, respectively, for the years 201, , etc., through All pairs are relatively fast moving, with mean motions of more than 6 yr OTS TO IDIVIDUAL ORBIT SYSTMS = FI 337BC = 42 Cet. The orbital period was determined using all data, but all other elements were determined by then fixing that period and using only speckle interferometry data. The measure of Tokovinin (1983) was given zero weight in the orbit solution. One historical unpublished CHARA measure is listed in Table 1 along with a very recent measure. Using the Hipparcos (Perryman et al. 1997) parallax and error from the more recent reduction of van Leeuwen (2007), the mass sum calculated from these elements, 1.79 ± 0.60 M, is consistent with the A7V (Bidelman 1958)of the secondary and a companion of unknown but likely similar type. The physical component A (G8III) is at 1. 6 from BC = HDS 787 = HD This is the first orbit solution for this pair. The mass sum predicted from these elements is 1.29 ± 0.44 M which is a little low for the F8+G8 pairing of Balega et al. (2002). The orbit can perhaps be substantially improved over the next several years, as it is predicted to pass quite quickly through periastron in = CHR 143Aa,Ab = HD Another first orbit, the very significant northern measure seen in Figure 1(c), is actually two measures. This pair should go through periastron soon (2013), but due to the higher eccentricity its motion is much more rapid as seen in Table 3. The mass sum derived from these elements is very uncertain: 27 ± 40 M. Adopting the mass sum 11.5 M appropriate for a B5V spectral type (Hiltner et al. 1969) and a slightly lower mass companion, we can derive a dynamical parallax 4.1 mas. The physical tertiary companion B is currently at from Aa,Ab = FI 348 = HD ot a first orbit, but the previous orbit (Mason & Hartkopf 2001) is not plotted due to scaling concerns. The mass sum predicted from these new elements is 4.3 ± 1.1 M, which is reasonably consistent with expectation for an A6/7III (Houk 1982) and a similar companion. ew measures (Mason et al. 2009; Paper I) found to the west in Figure 1(d) have demonstrated that the previous 470 yr period orbit was incorrect. The star is suspected to have variable radial velocity (ordstrom & Andersen 1985) = FI 297 AB = HD : The measure of McAlister & DeGioia (1979) was given zero weight in the orbit solution. The mass sum predicted from these elements is 0.93 ± 0.62 M, a bit low for an Am star and a fainter companion (Abt 1981). Compared to the previous orbits of Baize (1988) and Manté (2004b), the new orbit has a smaller a and P and fits the recent data much better. The tertiary component Cat12. 4 is physical = FI 370 = HD The mass sum calculated from new elements is 3.06 ± 0.68 M. Cutispoto et al. (2002) give the spectral type as G4IV/III+G2IV/III = FI 309 = HD Söderhjelm (1999) published elements with a period about twice those published here. The closer measures subsequently obtained resolved the quadrant ambiguity of other measures, yielding this shorterperiod solution. This solution also includes one unpublished USO speckle measure obtained in 2006 with the CTIO 4 m telescope. The mass sum is 2.50 ± 9 M and the spectral type from Abt (1981) isg1v = FI 372 = θ Cir. The mass sum is 40 ± 18 M. While the number of interferometric measures of this B3Ve (Slettebak 1982) star and its companion of unknown spectral type has doubled in the past 10 years, many more measures are needed = CHR 51 = 36 Ser. Two recent unpublished USO speckle measures made with the KPO 4 m and three CHARA speckle measures made with the Mt. Wilson 100 supplement the published data here. These are listed in Table 1. While a linear fit is also possible for these data (see Figure 4), definitive quadrant analysis of historical data (Bagnuolo et al. 1992) and recent measures of magnitude difference (Paper I) make it clear that the orbit solution (Figure 2(c)) is more likely to be correct. Three unpublished CHARA speckle measures were initially placed in the wrong quadrant leading to an erroneous solution in Hartkopf & Mason (2009). The final columns of Table 3 here provide the difference between the new orbit and that of Docobo & Tamazian (2009). The mass sum predicted from these new elements is 3.09 ± 0.47 M forthisa7+g0 pair (Faraggiana et al. 2004) = MCA 42C = β Sco. The relationships of the various components in this young high-order multiple system are illustrated in the mobile diagram in Figure 5. The measure of McAlister & DeGioia (1979) was given zero weight in the orbit solution. The orbit

4 Table 2 ew Orbital lements WDS Discoverer Desig. P a i Ω T 0 e ω Grade σ θ (deg) Previous σ θ (deg) (Figure o.) Other Desig. (yr) ( ) ( ) ( ) (yr) ( ) σ ρ (mas) Orbit σ ρ (mas) FI 337 BC Mason & Hartkopf (1999) 5.8 (1a) 42 Cet ±90 ±0071 ±2.8 ±17.0 ±3 ±11 ± HDS First orbit... (1b) HD ±0.36 ±040 ±4.0 ±3.5 ±6 ±24 ± CHR 143 Aa,Ab First orbit... (1c) HD ±5.4 ±17 ±2.4 ±6.9 ±8 ±8 ± FI Mason & Hartkopf (2001) 15.7 (1d) HD ±1.0 ±016 ±1.4 ±7.5 ±3 ±12 ± FI 297 AB Manté(2004a) 2.2 (1e) HD ±1.1 ±052 ±13.0 ±33.0 ±1.5 ±23 ± FI Manté(2004b) 4.9 (1f) HD ±5 ±034 ±5.9 ±13.0 ±0.32 ±23 ± FI Söderhjelm (1999) 3.1 (2a) HD ±21 ±021 ±2.6 ±4.1 ±55 ±051 ± FI Cvetkovíc (2009) 2.1 (2b) θ Cir ±0.78 ±0056 ±2.0 ±5.2 ±2 ±081 ± CHR Docobo & Tamazian (2009) 3.4 (2c) 36 Ser ±1.5 ±060 ±0.31 ±0.31 ±7 ±047 ± Hartkopf & Mason (2009) MCA 42 C Seymour et al. (2002) 12.7 (2d) β Sco ±2.9 ±060 ±9.0 ±14.0 ±9.9 ±57 ± FI Söderhjelm (1999) 2.7 (2e) HD ±50 ±043 ±1.1 ±0.62 ±7 ±048 ± MCA 53 Aa,Ab First orbit... (2f) 5 Aql ±0.78 ±16 ±1.4 ±1.9 ±0.76 ±54 ± CHR 88 Aa,Ab Hartkopf et al. (2000) 9.2 (3a) 45 Aql ±7 ±020 ±7.9 ±15.0 ±0.92 ±22 ± CHR Cvetkovíc (2009) 1.1 (3b) V505 Sgr ±1.1 ±11 ±14.0 ±13.0 ±0.85 ±69 ± FI Olevíc & Cvetkovíc (2003) 13.6 (3c) HD ±3.2 ±063 ±2.0 ±4.5 ±1.9 ±26 ± HDS Balega et al. (2006) 2.2 (3d) HD ±4.9 ±18 ±3.9 ±12.0 ±2.6 ±5 ± MCA Mason (1997) 5.8 (3e) 74 Aqr ±7 ±010 ±1.6 ±1.1 ±0.53 ±16 ± FI Docobo & Ling (2008) 2.5 (3f) 24 Psc ±5 ±014 ±1.8 ±2.7 ±4 ±13 ± o. 3, 2010 BIARY STAR ORBITS. IV. 737

5 738 MASO, HARTKOPF, & TOKOVII Vol. 140 WDS FI 337BC (a) WDS HDS 787 (b) WDS CHR 143Aa,Ab (c) WDS FI 348 (d) WDS FI 297AB (e) WDS FI 370 (f) Figure 1. ew orbits for the systems listed in Table 2, together with the most recent published elements for these systems and all data in the WDS database or Table 1. See the text for a description of symbols used in this and the following figures.

6 o. 3, 2010 BIARY STAR ORBITS. IV WDS FI 309 (a) 0WDS FI 372 (b) WDS CHR 51 (c) WDS MCA 42C (d) -0.3 WDS FI 355 (e) WDS MCA 53Aa,Ab (f) Figure 2. Same as Figure 1.

7 740 MASO, HARTKOPF, & TOKOVII Vol. 140 WDS CHR 88Aa,Ab (a) 0.4 WDS CHR 90 (b) WDS FI 336 (c) WDS HDS3053 (d) WDS MCA 73 (e) 0 WDS FI 359 (f) Figure 3. Same as Figure 1.

8 o. 3, 2010 BIARY STAR ORBITS. IV. 741 Table 3 Orbital phemerides WDS Discoverer Designation Designation θ ρ θ ρ θ ρ θ ρ θ ρ θ ρ FI 337 BC HDS CHR 143 Aa,Ab FI FI 297 AB FI FI FI CHR MCA 42 C FI MCA 53 Aa,Ab CHR 88 Aa,Ab CHR FI HDS MCA FI WDS CHR Figure 4. Linear fit to all speckle measures of 36 Ser (= = CHR 51), with quadrants of the recent data flipped by 180 as needed. The arrow at lower right indicates the direction of relative motion of the secondary; the dashed perpendicular line from the linear fit to the origin indicates the closest relative separation (71 mas, in ). This linear solution is less likely than the elliptical orbit depicted in Figure 2(c). of Holmgren et al. (1997), included in the mobile diagram, is of a much closer pair Aa,Ab, as is the orbit of Catanzaro (2010) for a,b. While the C component is a B2V (Johnson & Morgan 1953), recent analysis of the system (Catanzaro 2010) classified a as a mercury manganese star. The Aa,Ab orbit was obtained by combining spectroscopic and occultation data and provides the most accurate distance to this system through orbital parallax, π = 7.1 mas. This is in agreement with the Hipparcos parallax. However, adopting component s masses of C,a,b estimated from the spectral types (mass sum 18.6 M ), we obtain a discordant dynamical parallax of 4.4 mas from the new orbit. The visual orbit of AB with 610 yr period (Seymour et al. 2002) is suspect because it gives an even more discordant dynamical parallax. The available data only cover 1 3 of the calculated period. This interesting multiple system clearly deserves further study. The nomenclature of the components deserves some mention for this complex multiple system. As of the 1970s, four components of the multiple system were known. In van Flandern & spenschied (1975) they include the visual A, B, and C components noted above, as well as the 6.8 day spectroscopic companion, which they refer to as D. They then described the detection by lunar occultation of three more components: and F (both components of C) and G (a close component of B). While the G component was only postulated based on mass arguments, component F was implied from the detailed structure of the 1971 occultation by Io (Bartholdi & Owen 1972). The component designation was changed slightly in 1976 when lliott et al. (1975) redesignated the spectroscopic AD pair as A 1 A 2, a designation that was reinforced in vans et al. (1977). Following the protocols recommended by the IAU (Hartkopf & Mason 2004), the close spectroscopic pair is now known as Aa,Ab. It is quite likely that the F pair is the same as the day pair of Catanzaro (2010). The shifting components if nothing else give further evidence for the importance of clear nomenclature policy for stellar companions. In any event, the first speckle resolution of the close C pair followed so closely upon its first detection by occultation that the C designation was well established and was not designated Ca,Cb as might have been expected by modern schemes. The older designations of Ab [née A 2 (née D)] were historic and not retained. So, the complex multiple system is one without a D component = FI 355 = HD Recent measures have shown this pair to be closing in rather sooner than predicted by the orbit of Söderhjelm (1999). The mass sum of this high proper motion pair is 2.29 ± 6 M. The primary was classified as F9.5V in Gray et al. (2006) = MCA 53Aa,Ab = 5Aql.A first orbit determination for this pair is now possible due to the most recent measures, but this must be viewed as a very preliminary solution. The mass sum predicted from these elements is 13.0 ± 8.4 M

9 742 MASO, HARTKOPF, & TOKOVII Vol. 140 Figure 5. Mobile diagram of the β Sco (= ) multiple system. Table 4 System Parameters WDS Discoverer Parallax Spectral Mass Sum Designation Designation (mas) Type (M ) FI 337 BC 9.93 ± 1.03 A7V+? 1.79 ± HDS ± 1.19 F8+G ± CHR 143 Aa,Ab 3.12 ± 0.44 B5V+? 27.0 ± FI ± 0.37 A6/A7III+? 4.29 ± FI 297 AB 9.99 ± 1.68 Am+? 0.93 ± FI ± 0.65 G4IV/III+G2IV/III 3.06 ± FI ± 0.63 G1V 2.50 ± FI ± 9 B3Ve+? 4 ± CHR ± 0.33 A7+G ± MCA 42 C 8.19 ± 1.17 B2V+HgMn+? 2.9 ± FI ± 0.59 F9.5V+? 2.29 ± MCA 53 Aa,Ab 8.94 ± 1.14 Am+Am+? 13.0 ± CHR 88 Aa,Ab 9.26 ± 0.70 A3IV+? 1.87 ± CHR ± 0.57 A2V+F/GIV+F7V 9.6 ± FI ± 0.48 K1/2III+F 2.08 ± HDS ± 1.02 F8+G8 2.3 ± MCA ± 0.40 B8IV/V+?+? 23.1 ± FI ± 0.46 G9III+A0V 2.87 ± 0.56 for the pair of Am stars (Abt & Cardona 1984), although one of these components is also a double-lined spectroscopic binary with a 4.77 day period component (Abt & Levy 1985). The tertiary component B at is physical = CHR 88 Aa,Ab = 45 Aql. Measures in the northwest quadrant, not to become available for at least a decade, should significantly improve this fit. The current mass sum estimate of 1.87 ± 0.59 M is much lower than expected for a pair with A3IV primary (Cowley et al. 1969). However, Hipparcos detected an acceleration and its parallax measurement could be wrong. The faint red (V = 14.06, B V = 1.30) companion B at has common proper motion; it is physical = CHR 90 = V505 Sgr. Reassessing the position angle of the most recent observations yields a solution of approximately half the period and a much higher eccentricity than that of Cvetkovíc (2009). The mass sum predicted from these elements is 9.6 ± 4.4 M. The total mass of the brighter component, itself a 1.18 day spectroscopic and eclipsing binary composed of an A2V and a F/GIV, is 3.34 ± 4 M.The more distant speckle companion is probably of F7V spectral type (Tomkin 1992). Chambliss et al. (1993) estimate it to be 1.2 M. Our visual orbit leads then to the dynamical parallax of 10.8 mas, in agreement with the Hipparcos parallax of 8.6 ± 1.4 mas. The tertiary companion with an orbital period of 38.4 yr and high eccentricity was independently found by Mayer (1997)from the minima timings of the eclipsing pair. This early orbit roughly agrees with the present orbital solution. Recent work by Brož et al. (2010) postulated on a possible fourth companion and discussed the complex dynamics of the system = FI 336 = HD The orbital period was determined from all data, but all other elements were determined by fixing the period and using only speckle interferometry data. Two recent unpublished HRCam observations using the SOAR telescope, plus one made with the USO speckle camera on the KPO 4 m and one with the CHARA speckle camera on the Mt. Wilson 100, all supplement the published data here. The mass sum is 2.08 ± 0.84 M for the K1/2III+F

10 o. 3, 2010 BIARY STAR ORBITS. IV. 743 pair (Houk & Smith-Moore 1988). The quadrant was flipped for the 2009 HRCam observations = HDS3053 = HD The measure of Mason et al. (1999) made with the McDonald Observatory 82 is given zero weight in this orbit solution, which generates a predicted mass sum of 2.3 ± 2.2 M for the F8+G8 (Balega et al. 2002) pair. One recent unpublished HRCam observation and one USO speckle measure are included in Table = MCA 73 = 74 Aqr. A short-period, higheccentricity solution, which required flipping some measures by 180, was also attempted. However, the low-e solution consistent with the earlier orbit of Mason (1997) fits better and yields smaller errors. Periastron for this pair is predicted for Spring The mass sum is 23.1 ± 8.3 M. The visual primary is also a 3.43 day double-lined spectroscopic pair (Catanzaro & Leto 2004). The spectral classification of B8IV/ V (Houk & Smith-Moore 1988) is for the primary of this triple system = FI 359 = 24 Psc. A recent HRCam observation is included in Table 1. The mass sum predicted from these elements is 2.87 ± 0.73 M. The primary is a G9III while the secondary spectral type of A0V determined by Mason (1997) was based on the lunar occultation magnitude differences of vans & dwards (1981). Periastron for this pair is predicted for mid-2011, and multiple observations as it goes through this important phase can help refine its orbit further. Table 4 provides a summary of the parallax, spectral type, and mass sum for all these systems. Parallaxes are from the van Leeuwen (2007) Hipparcos reductions, while the spectral type information is a summary of that from the above-mentioned references. Due to the proximity of many of these pairs, the spectral type of the companion is often unknown; these are indicated by a? in Table 4. 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